This physical relationship between \(L_{\,\text{line}}\)  and \(L_{\text{\,acc}}\)  allows the estimation of the mass accretion rate (\(\dot{M}_{\text{\text{\,acc}}}\) ) [1]}. The \(\dot{M}_{\text{\,acc}}\)  of CTTSs was calculated by [2]} by analysing the excess UV and optical emission. A decade later, estimates of the \(\dot{M}_{\text{\,acc}}\)  for a large survey of young stars by [3]} was derived. Accretion through the disk is studied widely through shock models as well [4]}, [5]}, [6]}.
